The interstellar medium (ISM) refers to the material that fills the vast regions of space between stars within galaxies. It encompasses various components, including dust, thermal gas existing in different states (cold, warm, or hot, and ionized, neutral, or molecular), cosmic rays, and magnetic fields. One fascinating form of the ISM are molecular clouds. These dense and cold structures serve as favorable environments for star formation. This study aimed to investigate the interaction between ionized and neutral matter, as well as the magnetic field, within the molecular cloud Polaris Flare. We con ducted a comprehensive analysis of radio polarimetric measurements and radiation detected from the region at multiple frequencies. Synchrotron radiation at radio wavelengths proved to be a valuable tool for studying the ionized component of the ISM. We used observations of synchrotron radiation collected by the Low-Frequency Array (LOFAR) radiotelescope at low radio frequencies and performed a Faraday tomography on them using the rotation measurement (RM) synthesis technique. Our findings revealed a diffuse polarized emission structure characterized by straight depolarization canals. These canals represent regions where the polarized emission is absent. To gain insights into the 3D structure of the local magnetic field and the distribution of different types of matter within the cloud, we wanted to determine their orientations. For this purpose, we applied the Rolling Hough transform to both the LOFAR synchrotron radiation images and the neutral hydrogen maps obtained from the HI4PI survey. We also derived the plane-of-the-sky magnetic field orientations from starlight polarization data, collected by RoboPol using stellar optical polarimetry, and thermal dust emission captured by the Planck instruments. Upon analyzing the data, our results indicate a lack of correlation between the direction of the depolarization canals and the plane-of-the-sky magnetic field component. However, intriguing connections emerge between other components of the molecular cloud. In particular, we observe that the neutral hydrogen filaments at one speed interval show the same propagation direction as the detected depolarization canals. Furthermore, there is an overlap between the direction of propagation of the HI filaments at another speed interval and the magnetic field lines lying in the plane of the sky. These findings imply the possibility that correlating structures are localized within the same spatial portion of the molecular cloud.