  By studying the normalized cumulative radial distribution (nCRD) of the stars
in the central region of a Monte Carlo-simulated globular cluster, we recently
defined three parameters able to pinpoint the stage of internal dynamical
evolution reached by the system: $A_5$ (i.e., the area subtended by the nCRD
within 5$\%$ the half-mass radius, $r_h$), $P_5$ (the value of the nCRD at
5$\%$ $r_h$), and $S_{2.5}$ (the slope of the nCRD at 2.5$\%$ $r_h$). Here we
extend the analysis and explore the effects that different fractions (0$\%$,
10$\%$, and 20$\%$) of primordial binaries and stellar-mass black holes (BHs)
induce on the dynamical history of the system. As expected, the gradual
contraction of the cluster becomes milder and core collapse shallower for
increasing binary fraction. Nevertheless, the cluster dynamical evolution is
still properly traced by the three parameters. For models with a larger initial
retention of stellar mass BHs the evolution depends on the timescale of their
subsequent dynamical ejection. An early dynamical ejection of BHs results in a
long-term evolution of the three parameters similar to that found in systems
with no initial BH retention. Conversely, in the model that retains a large
number of BHs for extended time (slow dynamical ejection of BHs), the system is
characterized by a less concentrated structure and by the lack of significant
temporal evolution of the three parameters. The smaller values of the three
parameters found in this case might be used to indirectly infer the possible
presence of BHs in the cluster.
