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Our knowledge of relations between supermassive black holes and their host
galaxies at $z\gtrsim1$ is still limited, even though being actively sought out
to $z\sim6$. Here, we use the high resolution and sensitivity of JWST to
measure the host galaxy properties for 61 X-ray-selected type-I AGNs at
$0.7<z<2.5$ with rest-frame optical/near-infrared imaging from COSMOS-Web and
PRIMER. Black hole masses ($\log\left(M_{\rm BH}/M_\odot\right)\sim7.5-9.5$)
are available from previous spectroscopic campaigns. We extract the host galaxy
components from four NIRCam broadband images and the HST/ACS F814W image by
applying a 2D image decomposition technique. We detect the host galaxy for
$\sim90\%$ of the sample after subtracting the unresolved AGN emission. With
host photometry free of AGN emission, we determine the stellar mass of the host
galaxies to be $\log\left(M_*/M_\odot\right)\sim10-11.5$ through SED fitting
and measure the evolution of the mass relation between SMBHs and their host
galaxies. Considering selection biases and measurement uncertainties, we find
that the $M_\mathrm{ BH}/M_*$ ratio evolves as
$\left(1+z\right)^{0.37_{-0.60}^{+0.35}}$ thus remains essentially constant or
exhibits mild evolution up to $z\sim2.5$. We also see an amount of scatter
($\sigma_{\mu}=0.28\pm0.13$) is similar to the local relation and consistent
with low-$z$ studies; this appears to not rule out non-causal cosmic assembly
where mergers contribute to the statistical averaging towards the local
relation. We highlight improvements to come with larger samples from JWST and,
particularly, Euclid, which will exceed the statistical power of wide and deep
surveys such as Subaru Hyper Suprime-Cam.