  It has been proposed that the MACHOs in our galaxy could be clumped in
globular cluster--like associations or RAMBOs (robust associations of massive
baryonic objects) (Moore \& Silk 1995). Here we investigate the effect such
clustering has on the microlensing of stars in the Large Magellanic Cloud. We
find that the lensing in a one square degree field could be dominated by just a
few clusters. As a result the lensing properties vary widely depending on the
position and velocity of those clusters which happen to lie between us and the
LMC. Moreover we find a large variance in time scale distributions that
suggests that the small number statistics could easily be dominated by events
in the tails of the unclustered distribution ({\it e.g.} by long periods). We
compare our results with the MACHO collaboration's data and find that a
``standard'' halo made entirely of MACHOs is not strongly disfavored if the
clusters have masses of $10^6 M_{\odot}$. For less massive clusters such a halo
is not as likely. For $10^4 M_{\odot}$ clusters the microlensing statistics are
essentially unchanged from the unclustered case. It may be possible to detect
very massive clusters from the distribution of events in time-scale and space.
We provide some example time- scale distributions.
