  Over the last few decades, exhaustive surveys of extra Galactic globular
clusters (EGGCs) have become feasible. Only recently, kinematical information
of globular clusters (GCs) were available through Gaia DR2 spectroscopy and
also proper motions. On the other hand, simulations of GCs can provide detailed
information about the dynamical evolution of the system. We present a
preliminary study of EGGCs' properties for different dynamical evolutionary
stages. We apply this study to 12 Gyr-old GCs simulated as part of the MOCCA
Survey Database. Mimicking observational limits, we consider only a subssample
of the models in the database, showing that it is possible to represent
observed Galactic GCs. In order to distinguish between different dynamical
states of EGGCs, at least three structural parameters are necessary. The best
distinction is achieved by considering the central parameters, those being
observational core radius, central surface brightness, ratio between central
and half-mass velocity dispersion, or similarly considering the central color,
the central V magnitude and the ratio between central and half-mass radius
velocity dispersion, although such properties could be prohibitive with current
technologies. A similar but less solid result is obtained considering the
average properties at the half-light radius, perhaps accessible presently in
the Local Group. Additionally, we mention that the color spread in EGGCs due to
internal dynamical models, at fixed metallcity, could be just as important due
to the spread in metallicity.
