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% of 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 an 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 without initial BH retention. Conversely, in the model that retains a large number of BHs for an 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 lower values of the three parameters found in this case might be used to indirectly infer the possible presence of BHs in the cluster.
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