  In this work, we study some properties of the Hickson Compact Groups (HCGs)
using N-body simulations for the Generalized Dark Matter (GDM) model, described
by three free functions, the sound speed, the viscosity and the equation of
state. We consider three GDM models associated with different values of the
free functions to neglect collisional effects. We constructed the initial seeds
of our simulations according to the matter power spectrum of GDM linear
perturbations, which hold a cut-off at small scales, and explored their effects
on the non-linear structure formation at small and intermediate scales. We
generated mock catalogues of galaxies for different models and classify HCGs by
implementing an algorithm that adapts the original selection method for mock
catalogues. Once the HCGs samples are classified, we analyzed their properties
and compared them between models. We found that a larger amount of HCGs are
counted in GDM simulations in comparison to CDM counts. This difference
suggests that HCGs can proliferate within GDM despite the suppressed
substructure, which indicates a possible modification in the HCG formation
process within models where DM is not perfectly like CDM. Additionally, we
identified different mechanisms of clustering, for models with a large amount
of galaxy-halos self-agglomerate because of their abundance while models with
fewer galaxy-halos need massive halos acting as a dominant potential well.
Finally, by comparing distributions of different observables of simulated HCGs
against observations, we found a good agreement in the intrinsic properties.
However, a discrepancy in the velocity dispersion remains unsolved.
