We present 0”.2 (~80 au) resolution observations of the CO (2-1) and SiO (5-4) made with the Atacama millimeter/submillimeter array (ALMA) toward two extremely young intermediate-mass protostellar source, MMS 1 and MMS 6, located in the Orion Molecular Cloud 3 region (OMC-3). We first detected the molecular outflow and jet associated with MMS 1, which is a millimeter source without a bright infrared source wavelength shorter than 70 um. Our result shows clear evidence that MMS 1 already hosts a protostar. For both MMS 1 and MMS 6, we successfully resolved the compact protostellar jets, showing one-side lobe size of ~1000 au, in the SiO (5-4) emission for the first time. The detected jets have a very collimated structure (width of ~200 au) with the projected velocity up to ~50-60 km/s. The jets also show a wiggled structure, suggesting a precessing motion. The position-velocity (PV) diagrams of the jets obtained in SiO clearly showed the Hubble-like velocity structure, indicating that the SiO emission traces accelerated jets. Moreover, we confirmed that the SiO blue-shifted jet in MMS 1 contains three spatially resolved bullets. These bullets have different acceleration rates. The acceleration rate is larger for the inner bullet than the outer ones. The same tendencies such as the jet acceleration and different acceleration rates of blobs were found in the SiO blue-shifted jet in MMS 6. The bullet with different acceleration rates imply that the episodic mass ejection possibly occurs. We also confirmed the deacceleration of the bullet located at the tip of the jet, which can be explained by the interaction between the jet and the surrounding material.