  A subset of type Ic supernovae (SNe Ic), broad-lined SNe Ic (SNe Ic-bl), show
unusually high kinetic energies ($\sim 10^{52}$ erg) which cannot be explained
by the energy supplied by neutrinos alone. Many SNe Ic-bl have been observed in
coincidence with long gamma-ray bursts (GRBs) which suggests a connection
between SNe and GRBs. A small fraction of core-collapse supernovae (CCSNe) form
a rapidly-rotating and strongly-magnetized protoneutron star (PNS), a
proto-magnetar. Jets from such magnetars can provide the high kinetic energies
observed in SNe Ic-bl and also provide the connection to GRBs. In this work we
use the jetted outflow produced in a 3D CCSN simulation from a consistently
formed proto-magnetar as the central engine for full-star explosion
simulations. We extract a range of central engine parameters and find that the
extracted engine energy is in the range of $6.231 \times 10^{51}-1.725 \times
10^{52}$ erg, the engine time-scale in the range of $0.479-1.159$ s and the
engine half-opening angle in the range of $\sim 9-19^{\circ}$. Using these as
central engines, we perform 2D special-relativistic (SR) hydrodynamic (HD) and
radiation transfer simulations to calculate the corresponding light curves and
spectra. We find that these central engine parameters successfully produce SNe
Ic-bl which demonstrates that jets from proto-magnetars can be viable engines
for SNe Ic-bl. We also find that only the central engines with smaller opening
angles ($\sim 10^{\circ}$) form a GRB implying that GRB formation is likely
associated with narrower jet outflows and Ic-bl's without GRBs may be
associated with wider outflows.
