  The majority of binary star systems that host exoplanets will spend the first
portion of their lives within a star-forming cluster that may drive dynamical
evolution of the binary-planet system. We perform numerical simulations of
S-type planets, with masses and orbital architecture analogous to the solar
system's 4 gas giants, orbiting within the influence of a 0.5 solar-mass binary
companion. The binary-planet system is integrated simultaneously with an
embedded stellar cluster environment. ~10% of our planetary systems are
destabilized when perturbations from our cluster environment drive the binary
periastron toward the planets. This destabilization occurs despite all of our
systems being initialized with binary orbits that would allow stable planets in
the absence of the cluster. The planet-planet scattering triggered in our
systems typically results in the loss of lower mass planets and the excitement
of the eccentricities of surviving higher mass planets. Many of our planetary
systems that go unstable also lose their binary companions prior to cluster
dispersal and can therefore masquerade as hosts of eccentric exoplanets that
have spent their entire histories as isolated stars. The cluster-driven binary
orbital evolution in our simulations can also generate planetary systems with
misaligned spin-orbit angles. This is typically done as the planetary system
precesses as a rigid disk under the influence of an inclined binary, and those
systems with the highest spin-orbit angles should often retain their binary
companion and possess multiple surviving planets.
