  The ancient Large Magellanic Cloud (LMC) globular cluster NGC 2005 has
recently been reported to have an ex-situ origin, thus, setting precedents that
the LMC could have partially formed from smaller merged dwarf galaxies. We here
provide additional arguments from which we conclude that is also fairly
plausible an in-situ origin of NGC 2005, based on the abundance spread of a
variety of chemical elements measured in dwarf galaxies, their minimum mass in
order to form globular clusters, the globular cluster formation imprints kept
in their kinematics, and the recent modeling showing that explosions of
supernovae are responsible for the observed chemical abundance spread in dwarf
galaxies. The present analysis points to the need for further development of
numerical simulations and observational indices that can help us to
differentiate between two mechanisms of galaxy formation for the LMC, namely, a
primordial dwarf or an initial merging event of smaller dwarfs.
