  As ancient, gravitationally bound stellar populations, globular clusters are
abundant, vibrant laboratories characterized by high frequencies of dynamical
interactions coupled to complex stellar evolution. Using surface brightness and
velocity dispersion profiles from the literature, we fit $59$ Milky Way
globular clusters to dynamical models from the \texttt{CMC Cluster Catalog}.
Without doing any interpolation, and without any directed effort to fit any
particular cluster, $26$ globular clusters are well-matched by at least one of
our models. We discuss in particular the core-collapsed clusters NGC 6293, NGC
6397, NGC 6681, and NGC 6624, and the non-core-collapsed clusters NGC 288, NGC
4372, and NGC 5897. As NGC 6624 lacks well-fitting snapshots on the main
\texttt{CMC Cluster Catalog}, we run six additional models in order to refine
the fit. We calculate metrics for mass segregation, explore the production of
compact object sources such as millisecond pulsars, cataclysmic variables,
low-mass X-ray binaries, and stellar-mass black holes, finding reasonable
agreement with observations. Additionally, closely mimicking observational
cuts, we extract the binary fraction from our models, finding good agreement
except in the dense core regions of core-collapsed clusters. Accompanying this
paper are a number of \textsf{python} methods for examining the publicly
accessible \texttt{CMC Cluster Catalog}, as well as any other models generated
using \texttt{CMC}.
