  We present an analysis of the 3-D structure of the Magellanic Clouds, using
period-luminosity (P-L) relations of pulsating red giants in the OGLE-II
sample. By interpreting deviations from the mean P-L relations as distance
modulus variations, we examine the three-dimensional distributions of the
sample. The results for the Large Magellanic Cloud, based solely on stars below
the tip of the Red Giant Branch, confirm previous results on the inclined and
possibly warped bar of the LMC. The depth variation across the OGLE-II field is
about 2.4 kpc, interpreted as the distance range of a thin but inclined
structure. The inclination angle is about 29 deg. A comparison with OGLE-II red
clump distances revealed intriguing differences that seem to be connected to
the red clump reddening correction. A spatially variable red clump population
in the LMC can explain the deviations, which may have a broader impact on our
understanding of the LMC formation history. For the Small Magellanic Cloud, we
find a complex structure showing patchy distribution scattered within 3.2 kpc
of the mean. However, the larger range of the overall depth on every
line-of-sight is likely to smooth out significantly the real variations.
