  1ES1927+654 is a nearby active galactic nucleus that has shown an enigmatic
outburst in optical/UV followed by X-rays, exhibiting strange variability
patterns at timescales of months-years. Here we report the unusual X-ray, UV,
and radio variability of the source in its post-flare state (Jan 2022- May
2023). Firstly, we detect an increase in the soft X-ray (0.3-2 keV) flux from
May 2022- May 2023 by almost a factor of five, which we call the
bright-soft-state. The hard X-ray 2-10 keV flux increased by a factor of two,
while the UV flux density did not show any significant changes ($\le 30\%$) in
the same period. The integrated energy pumped into the soft and hard X-ray
during this period of eleven months is $\sim 3.57\times 10^{50}$ erg and
$5.9\times 10^{49}$ erg, respectively. From the energetics, it is evident that
whatever is producing the soft excess (SE) is pumping out more energy than
either the UV or hard X-ray source. Since the energy source presumably is
ultimately the accretion of matter onto the SMBH, the SE emitting region must
be receiving the majority of this energy. In addition, the source does not
follow the typical disc-corona relation found in AGNs, neither in the initial
flare (in 2017-2019) nor in the current bright soft state (2022-2023). We found
that the core (<1 pc) radio emission at 5 GHz gradually increased till March
2022 but showed a dip in August 2022. The G\"udel Benz relation ($L_{\rm
radio}/L_{\rm X-ray}\sim 10^{-5}$), however, is still within the expected range
for radio-quiet AGN and further follow-up radio observations are currently
being undertaken.
