  Thanks to ``dust-to-planet'' simulations (DTPSs), which treat the collisional
evolution directly from dust to giant-planet cores in a protoplanetary disk, we
showed that giant-planet cores are formed in $\lesssim 10\,$au in several
$10^5$ years, because porous pebbles grow into planetesimals via collisions
prior to drift in 10 au (Kobayashi & Tanaka 2021, Paper I).However, such porous
pebbles are unlikely to reproduce the polarized millimeter wavelength light
observed from protoplanetary disks. We thus investigate gas-giant core
formation with non-porous pebbles via DTPSs. Even non-porous bodies can grow
into planetesimals and massive cores to be gas giants are also formed in
several $10^5$ years. The rapid core formation is mainly via the accretion of
planetesimals produced by collisional coagulation of pebbles drifting from the
outer disk. The formation mechanism is similar to the case with porous pebbles,
while core formation occurs in a wider region (5 - 10 au) than that with porous
pebbles.
