  We investigate the formation of multiple-planet systems in the presence of a
hot Jupiter using extended N-body simulations that are performed simultaneously
with semi-analytic calculations. Our primary aims are to describe the planet
formation process starting from planetesimals using high-resolution
simulations, and to examine the dependences of the architecture of planetary
systems on input parameters (e.g., disk mass, disk viscosity). We observe that
protoplanets that arise from oligarchic growth and undergo type I migration
stop migrating when they join a chain of resonant planets outside the orbit of
a hot Jupiter. The formation of a resonant chain is almost independent of our
model parameters, and is thus a robust process. At the end of our simulations,
several terrestrial planets remain at around 0.1 AU. The formed planets are not
equal-mass; the largest planet constitutes more than 50 percent of the total
mass in the close-in region, which is also less dependent on parameters. In the
previous work of this paper (Ogihara et al. 2013), we have found a new physical
mechanism of induced migration of the hot Jupiter, which is called a
crowding-out. If the hot Jupiter opens up a wide gap in the disk (e.g., owing
to low disk viscosity), crowding-out becomes less efficient and the hot Jupiter
remains. We also discuss angular momentum transfer between the planets and
disk.
