  We explore the evolution of various properties of multiple-population
globular clusters (GCs) for a broad range of initial conditions. We simulated
over 200 GC models using the MOCCA Monte Carlo code and find that present-day
properties (core and half-light radii, ratio of the number of second-generation
(SG) stars to the total number of stars, NSG/NTOT) of these models cover the
observed values of these quantities for Milky Way GCs. Starting with a
relatively small value of the SG fraction (NSG/NTOT ~ 0.25) and a SG system
concentrated in the inner regions of the cluster, we find, in agreement with
previous studies, that systems in which the first-generation (FG) is initially
tidally filling or slightly tidally underfilling best reproduce the observed
ratios of NSG/NTOT and have values of the core and half-light radii typical of
those of many Galactic globular clusters. Models in which the FG is initially
tidally underfilling retain values of NSG/NTOT close to their initial values.
These simulations expand previous investigations and serve to further constrain
the viable range of initial parameters and better understand their influence on
present-day GC properties. The results of this investigation also provide the
basis for our future survey aimed at building specific models to reproduce the
observed trends (or lack thereof) between the properties of multiple stellar
populations and other clusters properties.
