  We present results on the recently discovered stellar system YMCA-1, for
which physical nature and belonging to any of the Magellanic System galaxies
have been irresolutely analyzed. We used SMASH and {\it Gaia} EDR3 data sets to
conclude that we are dealing with a small star cluster. Its reddening free,
field star decontaminated colour-magnitude diagram was explored in order to
obtain the cluster parameters. We found that YMCA-1 is a small (435
M$_{\odot}$), moderately old (age = 9.6 Gyr), moderately metal-poor ([Fe/H] =
-1.16 dex) star cluster, located at a nearly Small Magellanic Cloud (SMC)
distance (60.9 kpc) from the Sun, at $\sim$ 17.1 kpc to the East from the Large
Magellanic Cloud (LMC) centre. The derived cluster brightness and size would
seem to suggest some resemblance to the recently discovered faint star clusters
in the Milky Way (MW) outer halo, although it does not match their
age-metallicty relationship, nor those of MW globular clusters formed in-situ
or ex-situ, nor that of LMC clusters either, but is in agreement with that of
SMC old star clusters. We performed numerical Monte Carlo simulations
integrating its orbital motion backward in the MW-LMC-SMC system with radially
extended dark matter haloes that experience dynamical friction, and by
exploring different radial velocity (RV) regimes for YMCA-1. For RVs $\gtrsim$
300 km/s, the cluster remains bound to the LMC during the last 500 Myrs. The
detailed tracked kinematic of YMCA-1 suggests that its could have been stripped
by the LMC from the SMC during any of the close interactions between both
galaxies, a scenario previously predicted by numerical simulations.
