  In this work we study the Schwarzschild metric in the context of canonical
quantum gravity inside the horizon, close of horizon and near the black hole
singularity. Using this standard quantization procedure, we show that the
horizon is quantized and the black hole singularity disappears. For the first
case, quantization of the Schwarzschild radius was obtained in terms of the
Planck length $l_{Pl}$, a positive integer $n$ and the ordering factor of the
operator $p$. From the quantization of the Schwarzschild radius it was possible
to determine the area of the black hole event horizon, its mass and the quantum
energy of the Hawking radiation as well as its frequency. For the solution
close to the interior black hole singularity, the wave function was determined
and applied the DeBroglie-Bohm interpretation. The Bohm's trajectory was found
near to the singularity. It which describes how the spacetime evolves over time
and depends on the ordering factor of the operator $p$. Thus, for the case
where $|1-p|\neq0,3$, the Bohm's trajectory is finite and regular, that is, the
singularity is removed. For the case where $|1-p|=3$, the Bohm's trajectory
assumes an exponential behavior, never going to zero, avoiding the
singularity.That result allows that spacetime be extended beyond the classical
singularity.
