  We review the complications involved in the conversion of stellar
luminosities into masses and apply a range of mass-to-luminosity relations to
our Hubble Space Telescope observations of the young LMC star clusters NGC 1805
and NGC 1818.
  Both the radial dependence of the mass function (MF) and the dependence of
the cluster core radii on mass indicate clear mass segregation in both clusters
at radii r <= 20-30'', for masses in excess of ~1.6-2.5 Msun. This result does
not depend on the mass range used to fit the slopes or the metallicity assumed.
It is clear that the cluster MFs, at any radius, are not simple power laws.
  The global and the annular MFs near the core radii appear to be characterised
by similar slopes in the mass range (-0.15 <= log m/Msun <= 0.85), the MFs
beyond r >= 30'' have significantly steeper slopes.
  We estimate that while the NGC 1818 cluster core is between ~5 and ~30
crossing times old, the core of NGC 1805 is likely $\lesssim 3-4$ crossing
times old. However, since strong mass segregation is observed out to ~6 Rcore
and ~3 Rcore in NGC 1805 and NGC 1818, respectively, it is most likely that
significant primordial mass segregation was present in both clusters,
particularly in NGC 1805.
