  Numerical simulations have shown that black holes (BHs) can strongly
influence the evolution and present-day observational properties of globular
clusters (GCs). Using a Monte Carlo code, we construct GC models that match the
Milky Way (MW) cluster NGC 3201, the first cluster in which a stellar-mass BH
was identified through radial-velocity measurements. We predict that NGC 3201
contains $\gtrsim 200$ stellar-mass BHs. Furthermore, we explore the dynamical
formation of main sequence-BH binaries and demonstrate that systems similar to
the observed BH binary in NGC 3201 are produced naturally. Additionally, our
models predict the existence of bright blue-straggler-BH binaries unique to
core-collapsed clusters, which otherwise retain few BHs.
