  We report the identification of seven transient X-ray sources in the nearby
Magellanic-type galaxy NGC 4449 using the archival multi-epoch X-ray
observations conducted with {\it Chandra}, {\it XMM-Newton} and {\it Swift}
telescopes over year 2001--2013. Among them, two sources are classified as
supersoft X-ray sources (SSSs) because of their soft X-ray color and rest of
the sources are X-ray binaries (XRBs). Transient SSSs spectra can be fitted
with a blackbody of effective temperature $\sim 80-105$ eV and luminosities
were $\simeq 10^{37} - 10^{38} {\rm~erg\ s}^{-1}$ in 0.3--8 keV. These
properties are consistent with the widely accepted model for SSSs, an accreting
white dwarf with the steady nuclear burning on its surface, while the SSS
emission has also been observed in many post-nova systems. Detailed analysis of
one sufficiently bright SSS revealed the strong short-term variability,
possibly showing a 2.3 hour periodic modulation, and long-term variability,
detectable over 23 years with different X-ray telescopes before year 2003. The
X-ray properties of four other transients are consistent with neutron star or
black hole binaries in their hard state, while the remaining source is most
likely an XRB with a quasi-soft X-ray spectrum. Analysis of archival {\it
Hubble Space Telescope} image data was also conducted, and multiple massive
stars were found as possible counterparts. We conclude that the X-ray transient
properties in NGC 4449 are similar to those in other Magellanic-type galaxies.
