  Evidence of mutually inclined planetary orbits has been reported for giant
planets these last years. Here we aim to study the impact of eccentric and
inclined massive giant planets on the terrestrial planet formation process, and
investigate whether it can possibly lead to the existence of inclined
terrestrial planets. We have performed 126 simulations of the late-stage
planetary accretion in eccentric and inclined giant planet systems. The
physical and orbital parameters of the giant planet systems result from n-body
simulations of three giant planets in the late stage of the gas disc, under the
combined action of Type II migration and planet-planet scattering. Fourteen
two- and three-planet configurations have been selected, with diversified
masses, semi-major axes (resonant configurations or not), eccentricities and
inclinations (including coplanar systems) at the dispersal of the gas disc. We
have then followed the gravitational interactions of these systems with an
inner disc of planetesimals and embryos (9 runs per system), studying in detail
the final configurations of the formed terrestrial planets. While coplanar
giant systems harbour several terrestrial planets, generally as massive as the
Earth and mainly on low eccentric and low inclined orbits, terrestrial planets
formed in systems with mutually inclined giant planets are usually fewer, less
massive (<0.5 M_{\Earth}) and with larger eccentricities and inclinations. This
work shows that terrestrial planets can form on stable inclined orbits through
the classical accretion theory, even in coplanar giant planet systems emerging
from the disc phase.
