  Hot Jupiters generally do not have nearby planet companions, as they may have
cleared out other planets during their inward migration from more distant
orbits. This gives evidence that hot Jupiters more often migrate inward via
high-eccentricity migration due to dynamical interactions between planets
rather than more dynamically cool migration mechanisms through the
protoplanetary disk. Here we further refine the unique system of WASP-132 by
characterizing the mass of the recently validated 1.0-day period super-Earth
WASP-132c (TOI-822.02) interior to the 7.1-day period hot Jupiter WASP-132b.
Additionally, we announce the discovery of a giant planet at a 5-year period
(2.7 AU). We also detect a long-term trend in the radial velocity data
indicative of another outer companion. Using over nine years of CORALIE RVs and
over two months of highly-sampled HARPS RVs, we determine the masses of the
planets from smallest to largest orbital period to be M$_{\rm{c}}$ =
$6.26^{+1.84}_{-1.83}$ $M_{\oplus}$, M$_{\rm{b}}$ = $0.428^{+0.015}_{-0.015}$
$M_{\rm{Jup}}$, and M$_{\rm{d}}\sin{i}$ = $5.16^{+0.52}_{-0.52}$
$M_{\rm{Jup}}$, respectively. Using TESS and CHEOPS photometry data we measure
the radii of the two inner transiting planets to be $1.841^{+0.094}_{-0.093}$
$R_{\oplus}$ and $0.901^{+0.038}_{-0.038}$ $R_{\rm{Jup}}$. WASP-132 is a unique
multi-planetary system in that both an inner rocky planet and an outer giant
planet are in a system with a hot Jupiter. This suggests it migrated via a more
rare dynamically cool mechanism and helps to further our understanding of how
hot Jupiter systems may form and evolve.
