  We study dual AGN host galaxy morphologies at $z=2$ using the ASTRID
simulation, selecting black hole (BH) pairs with small separation ($\Delta
r<30\rm{kpc}$), high mass ($M_{\text{BH,12}}>10^7M_\odot$), and luminosity
($L_{\text{bol,12}}>10^{43}\rm{erg/s}$). We kinematically decompose (using
MORDOR) $\sim1000$ dual AGN hosts into standard components - a `disk' (thin and
thick disk, pseudo-bulge) and 'bulge' (bulge and halo) and define
disk-dominated galaxies by the disk-to-total $D/T\geq0.5$. In ASTRID,
$60.9\pm2.1\%$ of dual AGN hosts (independent of separation) are
disk-dominated, with the $D/T$ distribution peaking at $\sim0.7$. Notably,
hosts of BH pairs have similar morphologies (most either both disk or
bulge-dominated). In dual-AGN hosts, the $D/T$ increases from $\sim17\% $ at
$M_{\rm *}\sim 10^{9} M_{\odot}$ to $ 64\% $ for $M_{\rm *} \sim 10^{11.5}
M_{\odot}$, and the pseudo-bulge is the dominant component of the disk fraction
at the high mass end. Moreover, dual AGN hosts exhibit a higher fraction of
disk/large pseudo-bulge than single-AGN hosts. The Disk-to-Total ratio is
approximately constant with BH mass or AGN luminosity. We also create mock
images of dual AGN host galaxies, employing morphological fitting software
Statmorph to calculate morphological parameters and compare them with our
kinematic decomposition results. Around $83.3\pm2.4\%$ of galaxies display
disk-like profiles, of which $\sim60.7\pm2.2\%$ are kinematically confirmed as
disks. Se\'rsic indices and half-mass radii of dual AGN host galaxies align
with observational measurements from HST at $z\sim2$. Around $34\%$ are
identified as mergers from the $\text{Gini}-M_{20}$ relation. We find two dual
AGN hosted by galaxies that exhibit disk-like se\'rsic index $n_{12}<1$ and
$(D/T)_{12}>0.5$, which are in remarkable agreement with properties of recently
discovered dual quasars in disk galaxies at $z\sim 2$.
