  NGC 5033 is an intriguing Seyfert galaxy because its sub-classification may
change with time, and because optical and sub-mm observations find that the
massive black hole does not sit at the dynamical center of the galaxy, pointing
to a past merger. We obtained a new optical spectrum of NGC 5033 using the
200'' Hale telescope at Palomar that clearly reveals a broad H$\beta$ line
(FWHM$=5400\pm 300~{\rm km}~{\rm s}^{-1}$). This signals a clear view of the
optical broad line region (BLR) and requires Seyfert-1.5 designation. Some
spectra obtained in the past suggest a Seyfert-1.9 classification, potentially
signaling a variable or "changing-look" geometry. Our analysis of a 2019
Chandra spectrum of the massive black hole reveals very little obscuration,
also suggesting a clean view of the central engine. However, the narrow
Fe~K$\alpha$ emission line is measured to have an equivalent with of
EW$=460^{+100}_{-90}$~eV. This value is extremely high compared to typical
values in unobscured AGN. Indeed, the line is persistently strong in NGC 5033:
the line equivalent width in a 2002 XMM-Newton snapshot is
EW$=250^{+40}_{-40}$~eV, similar to the EW$=290^{+100}_{-100}$~eV equivalent
width measured using ASCA in 1999. These results can likely be explained
through a combination of an unusually high covering factor for reflection, and
fluxes that are seen out of phase owing to light travel times. We examine the
possibility that NGC 5033 may strengthen evidence for the X-ray Baldwin effect.
