We conducted wide-field (similar to 8' x 8') JHK(s) imaging polarimetric observations toward the massive star-formation region M 17. The southern H it bar is identified as large-scale infrared reflection nebula (IRN) illuminated by OB stars in the cluster center, while the northern bar shows polarization originating from dichroic extinction. Three small-scale bipolar IRN with centro-symmetric polarization patterns were identified, and their illuminating sources, embedded young stellar objects (YSOs), are most likely the driving sources of bipolar outflows. JHK(s) polarizations of point sources in M 17 show a wavelength dependence of the polarization of dichroic extinction in the general interstellar medium, indicating alpha similar to 1.8 for the empirical relation P proportional to lambda(-alpha) of interstellar polarization. The distribution of the polarization angle shows two peaks at 170 degrees and 110 degrees, indicating a non-uniform magnetic field structure in M 17. The direction of the magnetic field in the cluster region is south-north. However, the magnetic field in the HI! region is roughly between 100 degrees-140 degrees, roughly perpendicular to the Galactic disk. Such a configuration indicates that the magnetic field in the cluster region is twisted from the primordial orientation in the cluster formation. The magnetic field in the southern bar has a total strength of similar to 230 mu G, and is 40 degrees inclined to the plane of the sky. The outflows driven by YSOs in M 17 show a poor relation with the surrounding magnetic fields. This fact implies that the magnetic field in M 17 does not dominate the orientations of protostars formed inside.