  We have developed a new automated small-scale magnetic flux rope (SSMFR)
detection algorithm based on the Grad-Shafranov (GS) reconstruction technique.
We have applied this detection algorithm to the Wind spacecraft in-situ
measurements during 1996 - 2016, covering two solar cycles, and successfully
detected a total number of 74,241 small-scale magnetic flux rope events with
duration from 9 to 361 minutes. This large number of small-scale magnetic flux
ropes has not been discovered by any other previous studies through this unique
approach. We perform statistical analysis of the small-scale magnetic flux rope
events based on our newly developed database, and summarize the main findings
as follows. (1) The occurrence of small-scale flux ropes has strong solar cycle
dependency with a rate of a few hundreds per month on average. (2) The
small-scale magnetic flux ropes in the ecliptic plane tend to align along the
Parker spiral. (3) In low speed ($<$ 400 km/s) solar wind, the flux ropes tend
to have lower proton temperature and higher proton number density, while in
high speed ($\ge$ 400 km/s) solar wind, they tend to have higher proton
temperature and lower proton number density. (4) Both the duration and scale
size distributions of the small-scale magnetic flux ropes obey a power law. (5)
The waiting time distribution of small-scale magnetic flux ropes can be fitted
by an exponential function (for shorter waiting times) and a power law function
(for longer waiting times). (6) The wall-to-wall time distribution obeys double
power laws with the break point at 60 minutes (corresponding to the correlation
length). (7) The small-scale magnetic flux ropes tend to accumulate near the
heliospheric current sheet (HCS). The entire database is available at
\url{http://fluxrope.info} and in machine readable format in this article.
