We present infrared polarimetric images that demonstrate that the T Tauri star HL Tau is not seen in direct light at lambda <= 2.2 mu m. The position of the intensity centroid moves monotonically southwest from V (0.555 mu m) through J (1.25 mu m) and H (1.65 mu m) to K (2.2 mu m) wave bands. Furthermore, the mean position of the J, H, and K polarimetric centroids---which marks the position of the illuminating source of extensive reflection nebulosity---is displaced ~1" southwest of the position of the K-band intensity peak. This offset is in the same direction as the offset between the K-band intensity peak and the centroid of previously detected 3.6 cm emission. We conclude that, at optical and near-IR wavelengths, all of the observed radiation is scattered light from the circumstellar nebula. Our polarimetric images of HL Tau show a "polarization disk" at PA 134 deg and therefore support a model in which the projection of the equatorial plane of the protoplanetary disk is aligned at PA 134 deg. These results reinforce the contention that HL Tau is younger and more deeply embedded than typical T Tauri stars.