  We present a detailed exposition on the prospects of the formation of
Primordial Black Holes (PBHs) during Slow Roll (SR) to Ultra Slow Roll (USR)
sharp transitions in the framework of single-field inflation. We use an
effective field theory (EFT) approach in order to keep the analysis
model-independent and applicable to both the canonical and non-canonical cases.
We show in detail how renormalizing the power spectrum to one loop order in
$P(X,\phi)$ theories severely limits the prospects for PBH formation in a
single-field inflationary framework. We demonstrate that for the allowed range
of effective sound speed, $1<c_s<1.17$, the consistency of one-loop corrected
power spectrum leaves a small window for black hole masses, $M_{\rm PBH}\sim
\mathcal{O}(10^2-10^3)$gm to have sufficient e-foldings, $\Delta {\cal N}_{\rm
Total}\sim {\cal O}(54-59)$ for inflation. We confirm that adding an SR regime
after USR before the end of inflation does not significantly alter our
conclusions. Our findings for sharp transition strictly rule out the
possibility of generating large masses of PBHs from all possible models of
single-field inflation (canonical and non-canonical). Our results are at least
valid for the situation where constraints from the loop effects are computed
using either Late-Time (LT) or Adiabatic-Wave function (AF) scheme followed by
Power Spectrum (PS) renormalization schemes.
