  We confirm the existence of a second Large Magellanic Cloud (LMC) star
cluster, KMHK 1592, with an age that falls in the middle of the so-called LMC
star cluster age gap, a long period of time (~ 4 - 11 Gyr) where no star
cluster had been uncovered, except ESO121-SC03. The age (8.0+-0.5 Gyr) and the
metallicity ([Fe/H]=-1.0+-0.2 dex) of KMHK1592 were derived from the fit of
theoretical isochrones to the intrinsic star cluster colour-magnitude diagram
sequences, which were unveiled using a robust star-by-star membership
probability procedure. Because of the relative low brightness of the star
cluster, deep GEMINI GMOS images were used. We discuss the pros and cons of
three glimpsed scenarios that could explain the presence of both LMC age gap
star clusters in the outskirts of the LMC, namely: in-situ star cluster
formation, capture from the Small Magellanic Cloud, or accretion of a small
dwarf galaxy.
