  If ultra-high-energy cosmic rays (UHECRs) originate from extragalactic
sources, understanding the propagation of charged particles through the
magnetized large scale structure (LSS) of the universe is crucial in the search
for the astrophysical accelerators. Based on a novel model of the turbulence
dynamo, we estimate the intergalactic magnetic fields (IGMFs) in cosmological
simulations of the formation of the LSS. Under the premise that the sources of
UHECRs are strongly associated with the LSS, we consider a model in which
protons with E >10^{19} eV are injected by sources that represent active
galactic nuclei located inside clusters of galaxies. With the model IGMFs, we
then follow the trajectories of the protons, while taking into account the
energy losses due to interactions with the cosmic background radiation. For
observers located inside groups of galaxies like ours, about 70% and 35% of
UHECR events above 60 EeV arrive within ~15 degree and ~5 degree, respectively,
of the source position with time delays of less than ~10^7 yr. This implies
that the arrival direction of super-GZK protons might exhibit a correlation
with the distribution of cosmological sources on the sky. In this model, nearby
sources (within 10 - 20 Mpc) should contribute significantly to the particle
flux above ~10^{20} eV.
