  Swift J1818.0-1607 is a radio-loud magnetar with a spin period of 1.36 s and
a dipolar magnetic field strength of B~3E14 G, which is very young compared to
the Galactic pulsar population. We report here on the long-term X-ray
monitoring campaign of this young magnetar using XMM-Newton, NuSTAR, and Swift
from the activation of its first outburst in March 2020 until October 2021, as
well as INTEGRAL upper limits on its hard X-ray emission. The 1-10 keV magnetar
spectrum is well modeled by an absorbed blackbody with a temperature of
kT_BB~1.1 keV, and apparent reduction in the radius of the emitting region from
~0.6 to ~0.2 km. We also confirm the bright diffuse X-ray emission around the
source extending between ~50'' and ~110''. A timing analysis revealed large
torque variability, with an average spin-down rate nudot~-2.3E-11 Hz^2 that
appears to decrease in magnitude over time. We also observed Swift J1818.0-1607
with the Karl G. Jansky Very Large Array (VLA) on 2021 March 22. We detected
the radio counterpart to Swift J1818.0-1607 measuring a flux density of S_v =
4.38+/-0.05 mJy at 3 GHz, and a half ring-like structure of bright diffuse
radio emission located at ~90'' to the west of the magnetar. We tentatively
suggest that the diffuse X-ray emission is due to a dust scattering halo and
that the radio structure may be associated with the supernova remnant of this
young pulsar, based on its morphology.
