  We present a three-dimensional structure of the Magellanic System using over
9 000 Classical Cepheids and almost 23 000 RR Lyrae stars from the OGLE
Collection of Variable Stars. Given the vast coverage of the OGLE-IV data and
very high completeness of the sample, we were able to study the Magellanic
System in great details.
  We very carefully studied the distribution of both types of pulsators in the
Magellanic Bridge area. We show that there is no evident physical connection
between the Clouds in RR Lyrae stars distribution. We only see the two extended
structures overlapping. There are few classical Cepheids in the Magellanic
Bridge area that seem to form a genuine connection between the Clouds. Their
on-sky locations match very well young stars and neutral hydrogen density
contours. We also present three-dimensional distribution of classical pulsators
in both Magellanic Clouds.
