  We present results from photometric and spectroscopic data obtained with SOAR
and Gemini observatory facilities in the field of a recently discovered star
cluster. The cluster, projected towards the Eastern side of the outer disc of
the Large Magellanic Cloud (LMC), was originally placed nearly 10 kpc behind
the LMC with an age and metallicity typical of the innermost LMC star cluster
population. We assigned radial velocity (RV) memberships to stars observed
spectroscopically, and derived the cluster age and distance from theoretical
isochrone fitting to the cluster colour-magnitude diagram. The new object
turned out to be a 0.9 Gyr old outer LMC disc cluster, which possibly reached
the present position after being scattered from the innermost LMC regions where
it might have been born. We arrived at this conclusion by examining the spatial
distribution of LMC star clusters of similar age, by comparing the derived
spectroscopic metallicity with that expected for an outside-in galaxy formation
scenario, by considering the cluster internal dynamical stage as inferred from
its derived structural parameters and by estimating the circular velocity of a
disc that rotates with the corresponding star cluster radial velocity at the
cluster's deprojected distance, which resulted to be nearly 60 per cent higher
than that of most of the outer LMC disc clusters.
