  In this paper we study the gravitational lensing effect for the Schwarzschild
solution with holonomy corrections. We use two types of approximation methods
to calculate the deflection angle, namely the weak and strong field limits. For
the first method, we calculate the deflection angle up to the fifth order of
approximation and show the influence of the parameter $\lambda$ (in terms of
loop quantum gravity) on it. In addition, we construct expressions for the
magnification, the position of the lensed images and the time delay as
functions of the coefficients from the deflection angle expansion. We find that
$\lambda$ increases the deflection angle. In the strong field limit, we use a
logarithmic approximation to compute the deflection angle. We then write four
observables, in terms of the coefficients $b_1$, $b_2$ and $u_m$, namely: the
asymptotic position approached by a set of images $\theta_{\infty}$, the
distance between the first image and the others $s$, the ratio between the flux
of the first image and the flux of all other images $r_m$, and the time delay
between two photons $\Delta T_{2,1}$. We then use the experimental data of the
black hole Sagittarius $A^{\star}$ and calculate the observables and the
coefficients of the logarithmic expansion. We find that the parameter $\lambda$
increases the deflection angle, the separation between the lensed images and
the delay time between them. In contrast, it decreases the brightness of the
first image compared to the others.
