  We study the structures of ultra-relativistic jets injected into the
intracluster medium (ICM) and the associated flow dynamics, such as shocks,
velocity shear, and turbulence, through three-dimensional relativistic
hydrodynamic (RHD) simulations. To that end, we have developed a high-order
accurate RHD code, equipped with a weighted essentially non-oscillatory (WENO)
scheme and a realistic equation of state (Seo et al. 2021, Paper I). Using the
code, we explore a set of jet models with the parameters relevant to FR-II
radio galaxies. We confirm that the overall jet morphology is primarily
determined by the jet power, and the jet-to-background density and pressure
ratios play secondary roles. Jets with higher powers propagate faster,
resulting in more elongated structures, while those with lower powers produce
more extended cocoons. Shear interfaces in the jet are dynamically unstable,
and hence, chaotic structures with shocks and turbulence develop. We find that
the fraction of the jet-injected energy dissipated through shocks and
turbulence is greater in less powerful jets, although the actual amount of the
dissipated energy is larger in more powerful jets. In lower power jets, the
backflow is dominant in the energy dissipation owing to the broad cocoon filled
with shocks and turbulence. In higher power jets, by contrast, both the
backflow and jet spine flow are important for the energy dissipation. Our
results imply that different mechanisms, such as diffusive shock acceleration,
shear acceleration, and stochastic turbulent acceleration, may be involved in
the production of ultra-high energy cosmic rays in FR-II radio galaxies.
