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The velocity dispersion of globular clusters (GCs) around ultra-diffusegalaxies (UDGs) in the Virgo cluster spans a wide range, including cases whereGC kinematics suggest halos as massive as (or even more massive than) that ofthe Milky Way around these faint dwarfs. We analyze the catalogs of GCs derivedin post-processing from the TNG50 cosmological simulation to study the GCsystem kinematics and abundance of simulated UDGs in galaxy groups andclusters. UDGs in this simulation reside exclusively in dwarf-mass halos with$M_{200} \sim 10^{11}$ M$_{\odot}$. When considering only GCs gravitationallybound to simulated UDGs, we find GCs properties that overlap well with severalobservational measurements for UDGs. In particular, no bias towards overlymassive halos is inferred from the study of bound GCs, confirming that GCs aregood tracers of UDG halo mass. However, we find that contamination byintra-cluster GCs may, in some cases, substantially increase velocitydispersion estimates when performing projected mock observations of our sample.We caution that targets with less than $10$ GC tracers are particularly proneto severe uncertainties.Measuring the stellar kinematics of the host galaxyshould help confirm the unusually massive halos suggested by GC kinematicsaround some UDGs

Imposters among us: globular cluster kinematics and the halo mass of ultra-diffuse galaxies in clusters