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High-$z$ AGNs hosted in gas rich galaxies are expected to grow throughsignificantly obscured accretion phases. This may limit or bias theirobservability. In this work, we use \textsc{BlueTides}, a large volumecosmological simulation of galaxy formation to examine quasar obscuration forthe highest-redshift ($z \geq 7$) supermassive black holes residing in thecenter of galaxies. We find that for the bright quasars, most of the highcolumn density gas ($>90\%$) resides in the innermost regions of the hostgalaxy, (typically within $< 10$ ckpc), while the gas in the outskirts is aminor contributor to the $N_\mathrm H$. The brightest quasars can have largeangular variations in galactic obscuration, over 2 orders of magnitude, wherethe lines of sight with the lowest obscuration are those formed via strong gasoutflows driven by AGN feedback. We find that for the overall AGN population,the mean $N_\mathrm H$ is generally larger for high luminosity and BH mass,while the $N_\mathrm H$ distribution is significantly broadened, developing alow $N_\mathrm H $ wing due to the angular variations driven by the AGNoutflows/feedback. The obscured fraction P($N_{\rm H} > 10^{23} {\rm cm}^{-2}$)typically range from 0.6 to 1.0 for increasing $L_{X}$ (with $L_X > 10^{43}\rm{ergs/s}$), with no clear trend of redshift evolution. With respect to thegalaxy host property, we find a linear relation between $N_{\rm H}$, $M_*$ and$M_{\rm H_2}$ with $\log N_{\rm H} = (0.24 \pm 0.03) \log M_{*} + (20.7 \pm0.3)$ and $\log N_{\rm H} = (0.47 \pm 0.03) \log M_{\rm H_2} + (18.4 \pm 0.3)$.The dust optical depth in the UV band $\tau_{\mathrm UV}$ has tight positivecorrelation with $N_{\rm H}$. Our dust extincted UVLF is about 1.5 dex lowerthan the intrinsic UVLF, implying that more than 99\% of the $z \sim 7$ AGNsare heavily dust extincted and therefore would be missed by the UV bandobservation.

QSO obscuration at high redshift ($z \gtrsim 7$): Predictions from the BlueTides simulation