  It is clear that within the class of ultra-diffuse galaxies (UDGs) there is
an extreme range in the richness of their associated globular cluster (GC)
systems. Here, we report the structural properties of five UDGs in the Perseus
cluster based on deep Subaru / Hyper Suprime-Cam imaging. Three appear GC-poor
and two appear GC-rich. One of our sample, PUDG\_R24, appears to be undergoing
quenching and is expected to fade into the UDG regime within the next $\sim0.5$
Gyr. We target this sample with Keck Cosmic Web Imager (KCWI) spectroscopy to
investigate differences in their dark matter halos, as expected from their
differing GC content. Our spectroscopy measures both recessional velocities,
confirming Perseus cluster membership, and stellar velocity dispersions, to
measure dynamical masses within their half-light radius. We supplement our data
with that from the literature to examine trends in galaxy parameters with GC
system richness. We do not find the correlation between GC numbers and UDG
phase space positioning expected if GC-rich UDGs environmentally quench at high
redshift. We do find GC-rich UDGs to have higher velocity dispersions than
GC-poor UDGs on average, resulting in greater dynamical mass within the
half-light radius. This agrees with the first order expectation that GC-rich
UDGs have higher halo masses than GC-poor UDGs.
