  We seek to differentiate dynamical and morphological attributes between
globular clusters (GCs) that were formed inside their own dark matter (DM)
mini-halo, and those who were not. We employ high resolution full N-body
simulations on GPU of GCs with and without a DM mini-halo, orbiting a
Fornax-like dwarf galaxy. For GCs with DM, we observe that this dark extra mass
triggers a tidal radius growth that allows the mini-halo to act as a protective
shield against tidal stripping, being itself stripped beforehand the stars. We
demonstrate that this shielding effect becomes negligible when the tidal radius
is smaller than the half-mass radius of the mini-halo. Contrary to previous
predictions, we found that the inflation of outer stellar velocity dispersion
profiles is expected for GCs with and without a mini-halo, as a result of the
host's tidal field. Moreover, we observe that GCs with a DM mini-halo should
have, in general, relatively more radial outer velocity anisotropy profiles
throughout all their orbits, smaller degrees of internal rotation, and as a
consequence of the latter, smaller ellipticities for their stellar
distribution. Due to dynamical friction, we observe a clear bimodal
evolutionary distribution of GCs with and without DM in the integrals of motion
space and show that for GCs originally embedded in DM, this method is not
reliable for association with previous accretion events. Finally, we provide
parametric mass profiles of disrupted DM mini-halos from GCs to be used in
Jeans modelling and orbital integration studies.
