  We evaluate the effects of repulsive gravity using first order geometric
invariants, \textit{i.e.}, the Ricci scalar and the eigenvalues of the Riemann
curvature tensor, for three regular black holes, namely the Bardeen, Hayward,
and Dymnikova spacetimes. To examine the repulsive effects, we calculate their
respective onsets and regions of repulsive gravity. Afterwards, we compare the
repulsive regions obtained from these metrics among themselves and then with
the predictions got from the Reissner-Nordstr\"{o}m and Schwarzschild-de
Sitter. We find that the Dymnikova spacetime does not exhibit regions in which
gravity changes its sign. A notable characteristic, observed in all these
metrics, is that the repulsive regions appear to be unaffected by the mass that
generates the regular black hole. This property emerges due to the invariants
employed in our analysis, which do not change sign through \emph{linear
combinations} of the mass and the free coefficients of the metrics. As a
result, gravity can change sign independently of the specific values acquired
by the mass. This conclusion suggests a potential \emph{incompleteness} of
regular solutions, particularly in terms of their repulsive effects. To further
highlight this finding, we numerically compute, for the Reissner-Nordstr\"{o}m
and Schwarzschild-de Sitter solutions, the values of mass, $M$, that emulate
the repulsive effects found in the Bardeen and Hayward spacetimes. These
selected values of $M$ provide evidence that regular black holes do not
incorporate repulsive effects by means of the masses used to generate the
solutions themselves. Implications and physical consequences of these results
are then discussed in detail.
