  Small-scale interplanetary magnetic flux ropes (SMFRs) are similar to ICMEs
in magnetic structure, but are smaller and do not exhibit ICME plasma
signatures. We present a computationally efficient and GPU-powered version of
the single-spacecraft automated SMFR detection algorithm based on the
Grad-Shafranov (GS) technique. Our algorithm is capable of processing higher
resolution data, eliminates selection bias caused by a fixed $\avg{B}$
threshold, has improved detection criteria demonstrated to have better results
on an MHD simulation, and recovers full 2.5D cross sections using GS
reconstruction. We used it to detect 512,152 SMFRs from 27 years (1996 to 2022)
of 3-second cadence \emph{Wind} measurements. Our novel findings are: (1) the
radial density of SMFRs at 1 au (${\sim}1$ per $\si{10^6\kilo\meter}$) and
filling factor (${\sim}$35\%) are independent of solar activity, distance to
the heliospheric current sheet (HCS), and solar wind plasma type, although the
minority of SMFRs with diameters greater than ${\sim}$0.01 au have a strong
solar activity dependence; (2) SMFR diameters follow a log-normal distribution
that peaks below the resolved range ($\gtrsim 10^4$ km), although the filling
factor is dominated by SMFRs between $10^5$ to $10^6$ km; (3) most SMFRs at 1
au have strong field-aligned flows like those from PSP measurements; (4) in
terms of diameter $d$, SMFR poloidal flux $\propto d^{1.2}$, axial flux
$\propto d^{2.0}$, average twist number $\propto d^{-0.8}$, current density
$\propto d^{-0.8}$, and helicity $\propto d^{3.2}$. Implications for the origin
of SMFRs and switchbacks are briefly discussed. The new algorithm and SMFR
dataset are made freely available.
