  Using a Fourier-plane technique, we have merged HI ATCA and Parkes data sets
providing an accurate set of images of the LMC sensitive to structure on scales
of 15 pc (for an LMC distance of 55 kpc) upwards. The spatial dynamic range
(2.8 orders of magnitude), velocity resolution (1.649 km/s), brightness
temperature sensitivity (2.4 K) and column density sensitivity ($8.9 \times 10^
{18}$ cm$^{-2}$ per 1.649 km/s channel) allow for the studies of phenomena
ranging from the galaxy-wide interaction of the LMC with its close neighbours
to the small-scale injection of energy from supernovae and stellar associations
into the ISM of the LMC. We find that a previous analysis of the holes and
shells (Kim et al. 1999) in the HI distribution shows the same power- law
behavior with that of clumps. The measured perimeter P and measured enclosed
area A of each HI cloud in a log-log plot give us a set of points lying along
with a slope of D/2 = 0.73 $\pm$ 0.1. The relation between area and perimeter
of each identified HI cloud, P $\propto$ $A^{D/2}$, can determine the fractal
dimension D=1.47 $\pm$ 0.2 of a cloud boundary (Vogelaar & Wakker 1994;
Williams, Blitz, & McKee 2000). The measured fractal dimension of HI clouds in
the LMC is similar to the dimension, D=1.4, found in many studies of the
molecular ISM.
