The loop quantum dynamics of Kantowski-Sachs and Bianchi-III LRS spacetimes with cosmological constant is studied in the effective spacetime description. We show that classical singularity is avoided, and replaced by bounces of the triads. Unlike the singularity resolution in other loop quantum spacetimes, evolution results in a spacetime which retains quantum curvature after the bounce on one side of the temporal evolution. In the asymptotic limit, a spacetime which is a direct product of two constant curvature spaces emerges. Interestingly, despite high curvature, the effective spacetime metric is a solution of Einstein field's equations albeit with a different stress energy tensor. For the Kantowski-Sachs case, the resulting spacetime is a 'charged' Nariai spacetime, and for the Bianchi-III LRS spacetime, one obtains anti-Bertotti-Robinson spacetime with an emergent cosmological constant. The emergent 'charge' and cosmological constant are purely quantum geometric in origin.Keywords: Loop quantum cosmology; black hole interiors.Using techniques of loop quantum gravity, quantization of various homogenous spacetimes has been performed recently in loop quantum cosmology (LQC) 2 . One of the main results is the resolution of big bang singularity and occurrence of bounce at the Planck scale 3 . For the cosmological models, such as the isotropic homogeneous spacetime or Bianchi models, at small curvatures, far from the bounce, dynamics can be approximated extremely well by the classical Hamiltonian evolution of the respective spacetimes. Quantum gravitational effects are important only in a small regime near the bounce. For an exactly solvable model in LQC 4 , the properties of the spacetime across the bounce are almost identical 5 . Extension of these results on singularity resolution has been investigated for the black hole spacetimes 6-10 . It has been generally expected that as in the case of isotropic model in LQC, the spacetime after the bounce in the black hole interior shares very similar properties as the one before the bounce. Recent studies 1,10 , show that this expectation does not hold. For the Kantowski-Sachs spacetime which captures the interior of Schwarzschild black hole and the Bianchi-III LRS spacetime which is isomorphic to higher genus black hole interior, the central singularity is resolved, but the spacetime on one side of the temporal evolution is drastically different from the initial classical spacetime. It turns out that quantum geometric effects do not die, and remain significant even asymptotically, leading to an emergent spacetime metric * Anton Joe passed away before results in this manuscript and its earlier expanded version 1 were communicated. ND and PS dedicate this article to Anton Joe.