  Most stars in our Galaxy form in stellar aggregates, which can become
long-lived structures called open clusters (OCs). Along their dynamical
evolution, their gradual depletion leave some imprints on their structure. In
this work, we employed astrometric, photometric and spectroscopic data from the
\textit{Gaia} DR3 catalogue to uniformly characterize a sample of 60 OCs.
Structural parameters (tidal, core and half-light radii, respectively, $r_t$,
$r_c$ and $r_h$), age, mass ($M_{\textrm{clu}}$), distance, reddening, besides
Jacobi radius ($R_J$) and half-light relaxation time ($t_{rh}$), are derived
from radial density profiles and astrometrically decontaminated
colour-magnitude diagrams. Ages and Galactocentric distances ($R_G$) range from
7.2$\,\lesssim\,$log($t.$yr$^{-1}$)$\,\lesssim\,$9.8 and
6$\,\lesssim\,R_G$(kpc)$\,\lesssim\,$12. Analytical expressions derived from
$N$-body simulations, taken from the literature, are also employed to estimate
the OC initial mass ($M_{\textrm{ini}}$) and mass loss due to exclusively
dynamical effects. Both $r_c$ and the tidal filling ratio, $r_h/R_J$, tend to
decrease with the dynamical age (=$t/t_{rh}$), indicating the shrinking of the
OCs' internal structure as consequence of internal dynamical relaxation. This
dependence seems differentially affected by the external tidal field, since OCs
at smaller $R_G$ tend to be dynamically older and have smaller
$M_{\textrm{clu}}/M_{\textrm{ini}}$ ratios. In this sense, for
$R_G\lesssim8\,$kpc, the $r_h/R_J$ ratio presents a slight positive correlation
with $R_G$. Beyond this limit, there is a dichotomy in which more massive OCs
tend to be more compact and therefore less subject to tidal stripping in
comparison to those less massive and looser OCs at similar $R_G$. Besides, the
$r_t/R_J$ ratio also tends to correlate positively with $R_G$.
