  One intriguing approach for studying the dynamical evolution of galaxy
clusters is to compare the spatial distributions among various components, such
as dark matter, member galaxies, gas, and intracluster light (ICL). Utilizing
the recently introduced Weighted Overlap Coefficient (WOC)
\citep{2022ApJS..261...28Y}, we analyze the spatial distributions of components
within 174 galaxy clusters ($M_{\rm tot}> 5 \times 10^{13} M_{\odot}$,
$z=0.625$) at varying dynamical states in the cosmological hydrodynamical
simulation Horizon Run 5. We observe that the distributions of gas and the
combination of ICL with the brightest cluster galaxy (BCG) closely resembles
the dark matter distribution, particularly in more relaxed clusters,
characterized by the half-mass epoch. The similarity in spatial distribution
between dark matter and BCG+ICL mimics the changes in the dynamical state of
clusters during a major merger. Notably, at redshifts $>$ 1, BCG+ICL traced
dark matter more accurately than the gas. Additionally, we examined the
one-dimensional radial profiles of each component, which show that the BCG+ICL
is a sensitive component revealing the dynamical state of clusters. We propose
a new method that can approximately recover the dark matter profile by scaling
the BCG+ICL radial profile. Furthermore, we find a recipe for tracing dark
matter in unrelaxed clusters by including the most massive satellite galaxies
together with BCG+ICL distribution. Combining the BCG+ICL and the gas
distribution enhances the dark matter tracing ability. Our results imply that
the BCG+ICL distribution is an effective tracer for the dark matter
distribution, and the similarity of spatial distribution may be a useful probe
of the dynamical state of a cluster.
