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Optical secondary eclipse measurements made by \emph{Kepler} reveal a diverseset of geometric albedos for hot Jupiters with equilibrium temperatures between$1550-1700$ K. The presence or absence of high altitude condensates, such asMg$_2$SiO$_4$, Fe, Al$_2$O$_3$, and TiO$_2$, can significantly alter opticalalbedos, but these clouds are expected to be confined to localized regions inthe atmospheres of these tidally locked planets. Here, we present 3D generalcirculation models and corresponding cloud and albedo maps for six hot Jupiterswith measured optical albedos in this temperature range. We find that theobserved optical albedos of K2-31b and K2-107b are best matched by either cloudfree models or models with relatively compact cloud layers, while Kepler-8b andKepler-17b's optical albedos can be matched by moderately extended ($f_{sed}$ =0.1) parametric cloud models. HATS-11b has a high optical albedo, correspondingto models with bright Mg$_2$SiO$_4$ clouds extending to very low pressures($f_{sed}$ = 0.03). We are unable to reproduce Kepler-7b's high albedo, as ourmodels predict that the dayside will be dominated by dark Al$_2$O$_3$ clouds atmost longitudes. We compare our parametric cloud model with a two-zonemicrophysical cloud model (\texttt{CARMA}). We find that even after accountingfor the 3D thermal structure, no single cloud model can explain the full rangeof observed albedos within the sample. We conclude that a better knowledge ofthe vertical mixing profiles, cloud radiative feedback, cloud condensateproperties, and atmospheric metallicities is needed in order to explain theunexpected diversity of albedos in this temperature range.

Spatially Resolved Modeling of Optical Albedos for a Sample of Six Hot Jupiters