  We present the photometric and spectroscopic evolution of supernova (SN)
2019cad during the first $\sim100$ days from explosion. Based on the light
curve morphology, we find that SN 2019cad resembles the double-peaked type Ib/c
SN 2005bf and the type Ic PTF11mnb. Unlike those two objects, SN 2019cad also
shows the initial peak in the redder bands. Inspection of the g-band light
curve indicates the initial peak is reached in $\sim8$ days, while the r band
peak occurred $\sim15$ days post-explosion. A second and more prominent peak is
reached in all bands at $\sim45$ days past explosion, followed by and fast
decline from $\sim60$ days. During the first 30 days, the spectra of SN 2019cad
show the typical features of a type Ic SN, however, after 40 days, a blue
continuum with prominent lines of Si II ${\lambda}6355$ and C II
${\lambda}6580$ is observed again. Comparing the bolometric light curve to
hydrodynamical models, we find that SN 2019cad is consistent with a pre-SN mass
of 11 M$_{\odot}$, and an explosion energy of $3.5\times 10^{51}$ erg. The
light curve morphology can be reproduced either by a double-peaked $^{56}$Ni
distribution with an external component of 0.041 M$_{\odot}$ and an internal
component of 0.3 M$_{\odot}$ or a double-peaked $^{56}$Ni distribution plus
magnetar model (P $\sim11$ ms and B $\sim26\times 10^{14}$ G). If SN 2019cad
were to suffer from significant host reddening (which cannot be ruled out), the
$^{56}$Ni model would require extreme values, while the magnetar model would
still be feasible.
