  The dust in planet-forming disks evolve rapidly through growth and radial
drift, and external photoevaporation also contributes to this evolution in
massive star-forming regions. We test whether the presence of substructures can
explain the survival of the dust component and observed millimeter continuum
emission in protoplanetary disks located within massive star-forming regions.
We also characterize the dust content removed by the photoevaporative winds.
For this, we performed hydrodynamical simulations of protoplanetary disks
subject to irradiation fields of $F_{UV} = 10^2$, $10^3$, and $10^4\, G_0$,
with different dust trap locations. We used the FRIED grid to derive the mass
loss rate for each irradiation field and disk properties, and then measure the
evolution of the dust mass over time. For each simulation we estimate continuum
emission at $\lambda = 1.3\, \textrm{mm}$ along with the radii encompassing
$90\%$ of the continuum flux, and characterize the dust size distribution
entrained in the photoevaporative winds, along with the resulting
far-ultraviolet (FUV) cross section. Our simulations show that the presence of
dust traps can extend the lifetime of the dust component of the disk to a few
millionyears if the FUV irradiation is $F_{UV} \lesssim 10^3 G_0$, but only if
the dust traps are located inside the photoevaporative truncation radius. The
dust component of a disk quickly disperse if the FUV irradiation is strong
($10^4\, G_0$) or if the substructures are located outside the photoevaporation
radius. We do find however, that the dust grains entrained with the
photoevaporative winds may result in an absorption FUV cross section of $\sigma
\approx 10^{-22}\, \textrm{cm}^2$ at early times of evolution ($<$0.1 Myr),
which is enough to trigger a self-shielding effect that reduces the total mass
loss rate, and slow down the disk dispersal in a negative feedback loop
process.
