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In this work we study the Schwarzschild metric in the context of canonicalquantum gravity inside the horizon, close of horizon and near the black holesingularity. Using this standard quantization procedure, we show that thehorizon is quantized and the black hole singularity disappears. For the firstcase, quantization of the Schwarzschild radius was obtained in terms of thePlanck length $l_{Pl}$, a positive integer $n$ and the ordering factor of theoperator $p$. From the quantization of the Schwarzschild radius it was possibleto determine the area of the black hole event horizon, its mass and the quantumenergy of the Hawking radiation as well as its frequency. For the solutionclose to the interior black hole singularity, the wave function was determinedand applied the DeBroglie-Bohm interpretation. The Bohm's trajectory was foundnear to the singularity. It which describes how the spacetime evolves over timeand depends on the ordering factor of the operator $p$. Thus, for the casewhere $|1-p|\neq0,3$, the Bohm's trajectory is finite and regular, that is, thesingularity is removed. For the case where $|1-p|=3$, the Bohm's trajectoryassumes an exponential behavior, never going to zero, avoiding thesingularity.That result allows that spacetime be extended beyond the classicalsingularity.

Quantization of the interior of the black hole