  We study the intracluster light (ICL) and intracluster globular clusters
(ICGCs) in the nearby Perseus galaxy cluster using Euclid's EROs. By modelling
the isophotal and iso-density contours, we map the distributions and properties
of the ICL and ICGCs out to a radius of 600 kpc (~1/3 of the virial radius)
from the brightest cluster galaxy (BCG). We find that the central 500 kpc of
the Perseus cluster hosts 70000$\pm$2800 GCs and $1.6\times10^{12}$ L$_\odot$
of diffuse light from the BCG+ICL in the near-infrared H$_E$. This accounts for
37$\pm$6% of the cluster's total stellar luminosity within this radius. The ICL
and ICGCs share a coherent spatial distribution, suggesting a common origin or
that a common potential governs their distribution. Their contours on the
largest scales (>200 kpc) are offset from the BCG's core westwards by 60 kpc
towards several luminous cluster galaxies. This offset is opposite to the
displacement observed in the gaseous intracluster medium. The radial surface
brightness profile of the BCG+ICL is best described by a double S\'ersic model,
with 68$\pm$4% of the H$_E$ light in the extended, outer component. The
transition between these components occurs at ~50 kpc, beyond which the
isophotes become increasingly elliptical and off-centred. The radial ICGC
number density profile closely follows the BCG+ICL profile only beyond this 50
kpc radius, where we find an average of 60 GCs per $10^9$ M$_\odot$ of diffuse
stellar mass. The BCG+ICL colour becomes increasingly blue with radius,
consistent with the stellar populations in the ICL having subsolar
metallicities [Fe/H]~-0.6. The colour of the ICL, and the specific frequency
and luminosity function of the ICGCs suggest that the ICL+ICGCs were tidally
stripped from the outskirts of massive satellites with masses of a few
$\times10^{10}$ M$_\odot$, with an increasing contribution from dwarf galaxies
at large radii.
